We demonstrated our new procedure by means of a simple example, i.e., the GW signal from the electroweak phase transition in the real-scalar-singlet extension of the Standard Model (xSM).
The main results of our analysis are shown in Figs. REF  and REF .
These plots represent a projection of a sample of viable xSM parameter points into the space of peak frequencies and peak amplitudes.
The experimental sensitivities of upcoming GW observatories are illustrated by what we call peak-integrated sensitivity curves (PISCs) in these plots; see Eq. (REF ).
Specifically, we presented the PISCs of three future space-based GW interferometers: LISA, DECIGO, and BBO.
A more detailed discussion of these sensitivity curves can be found in the companion paper [1]}.
The main message from our PISC plots in Figs. REF  and REF  is that they provide a bird's eye view of the GW phenomenology of the xSM.
Not only do our PISC plots allow us to assess which parts of the xSM signal region will be probed by LISA, DECIGO, and BBO, respectively, they also set the stage for the study of underlying model-parameter dependencies as well as for the construction of histograms that reflect the relative rate of occurrence of particular peak frequencies and peak amplitudes.
